We also briefly compare our absorption-modified \(\dot{M}\) –\({L_{\textnormal {H}\,\alpha }} \)  relationship to the fit of [1]} for CTTSs.
A detailed comparison, including a discussion of the physical differences, is given in [2]}.
Up to \(\dot{M} \sim 10^{-5.5}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\)  for SpherAcc and Polar, and up to \(\dot{M} \sim 10^{-6.5}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\)  for MagAcc, the slopes are similar between the linear fit and our curves, but with a significant offset of approximately 1.5 dex (several times the spread \(\sigma \approx 0.5\)  dex of the fit of [1]}). At large accretion rates, the difference grows dramatically. This implies that a given observed H \(\alpha \)  luminosity requires much more vigorous accretion in planets than in stars.
